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The O Star Hinterland of the Galactic Starburst, NGC 3603

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The O Star Hinterland of the Galactic Starburst, NGC 3603 MNRAS 000, 000{000 (0000) Preprint 22 March 2019 Compiled using MNRAS LATEX style file v3.0 The O star hinterland of the Galactic starburst, NGC 3603 J. E. Drew1?, M. Mongui´o1, N. J. Wright2 1School of Physics, Astronomy & Mathematics, University of Hertfordshire, Hatfield AL10 9AB, UK 2Astrophysics Group, Keele University, Keele, ST5 5BG, UK 22 March 2019 ABSTRACT The very bright and compact massive young cluster, NGC 3603, has been cited as an example of a starburst in the Milky Way and compared with the much-studied R136/30 Doradus region in the Large Magellanic Cloud. Here we build on the discovery by Mohr-Smith et al.(2017) of a large number of reddened O stars around this cluster. We construct a list of 288 candidate O stars with proper motions, in a region of sky spanning 1:5×1:5 square degrees centered on NGC 3603, by cross-matching the Mohr- Smith et al. (2017) catalogue with Gaia DR2 (Gaia Collaboration et al. 2018). This provides the basis for a first comprehensive examination of the proper motions of these massive stars in the halo of NGC 3603, relative to the much better studied central region. We identify up to 11 likely O star ejections { 8 of which would have been ejected between 0.60 and 0.95 Myr ago (supporting the age of ∼1 Myr that has been attributed to the bright cluster centre). Seven candidate ejections are arranged in a partial ring to the south of the cluster core spanning radii of 9{18 arcmin (18{36 pc if the cluster is 7 kpc away). We also show that the cluster has a halo of a further ∼100 O stars extending to a radius of at least 5 arcmin, adding to the picture of NGC 3603 as a scaled down version of the R136/30 Dor region. Key words: stars: early-type, (Galaxy:) open clusters and associations: NGC 3603, Galaxy: structure, surveys 1 INTRODUCTION dense and massive clusters in the Milky Way. Indeed, the ex- treme stellar density in the core has prompted comparisons Massive young clusters are rare objects that nevertheless ex- with the extragalactic starburst phenomenon (e.g. Eisen- ert a major influence on their galactic environments. Their hauer et al. 1998; Moffat et al. 2002; Stolte et al. 2006). The modes of formation remain an important topic of research, mass of the cluster is among the highest measured in the echoing continuing significant uncertainty in the modes of Milky Way: Harayama et al.(2008) placed it in the range evolution of the most massive stars that are their distinctive from 10 000 up to 16 000 M , while Rochau et al.(2010) constituents. Clues to the early internal dynamics of massive obtained ∼18 000 M . The age often cited for NGC 3603, young clusters can come from the O stars they eject (Fujii & based on the stellar content of its inner core of diameter Portegies Zwart 2011). With the arrival of Gaia DR2 proper ∼ 20 arcsec is 1 to 2 Myr (e.g. Sung & Bessell 2004; Melena arXiv:1903.09053v1 [astro-ph.SR] 21 Mar 2019 motions and the availability of wide field photometric sur- et al. 2008; Kudryavtseva et al. 2012). This core is some- veys, the opportunity now exists to locate ejected O stars times referred to as the HD 97950 cluster. Measurements in the environs of their birth clusters. In a previous paper over a wider sky area out to a radius of an arcminute or so, (Drew et al. 2018) we studied the example of Westerlund have indicated that an older, lower density population may 2 and discovered a surprisingly ordered 'twin-exhaust' pat- be present as well (Melena et al. 2008; Beccari et al. 2010). tern of ejections that may favour the creation of Westerlund 2 via the merger of distinct sub-clusters. Here we move on In earlier work (Mohr-Smith et al. 2015, 2017, here- to the example of NGC 3603, the even brighter and more after MS-I and MS-II), we presented blue selections of OB compact clustering in the region. stars from the VST Photometric Hα Survey of the South- Like Westerlund 2, NGC 3603 is in the Carina region ern Galactic Plane and Bulge (VPHAS+, Drew et al. 2014) of the Galactic Plane. It is one of a small number of very across the Carina region, and showed that their conversion to spectroscopically-confirmed OB stars is very high. The MS-II list of 5915 O-B2 candidates is accompanied by high- ? E-mail: [email protected] quality measures of extinction, along with estimates of ef- c 0000 The Authors 2 J. E. Drew et al fective temperatures that are good enough to broadly clas- sify as early-O, later-O and early-B stars. These are derived from fitting each object's spectral energy distribution (SED) 150 as represented by its u=g=r=i=J=H=K magnitudes. Here, we reuse MS-II in order to focus on the hinterland of NGC 3603. This paper is organised as follows. First, we select from 100 MS-II a set of high-confidence O stars within a region of 1.5×1.5 sq.deg centred on NGC 3603, and crossmatch it with the Gaia DR2 database (Gaia Collaboration et al. 2018) with the aim of utilising the proper motion (PM) data (Sec- 50 tion2). We then compute the mean proper motion of the cluster using stars located within 1 arcminute of the cluster centre which becomes the basis for relative proper motions 0 (rPM, see sections 4.1 and 4.2). This enables the identifica- 4.2 4.3 4.4 4.5 4.6 tion of probable cluster escapes that turn out, intriguingly, log(Teff K) to be located in a half ring (section 4.3). After some sam- 140 ple decontamination, we consider the radial distribution of the O star candidates and find it largely follows the King 120 model adopted by Harayama et al.(2008). The paper ends with a discussion of the significance of the results and some 100 conclusions (sections6 and7). 80 60 2 CONSTRUCTION OF THE SAMPLE 40 We adopt as the central reference position in the core of 20 NGC 3603 the Galactic coordinates, ` = 291◦:617, b = ◦ −0 :523. The selection box on the sky around this posi- 0 tion is a square occupying 1.5×1.5 deg2, with sides oriented 0 1 2 3 4 5 6 7 8 9 10 along the directions of constant Galactic longitude and lati- extinction (A0) tude. Within this region, the MS-II database provides a list of 1663 blue-selected OB candidate stars. Of these we retain 100 as a long list those objects for which the reported quality 2 of fits to their optical-NIR SEDs is χ < 25. MS-II recom- 80 mended a tighter χ2 limit than this for the selection of "good OB stars": it is relaxed here so as not to exclude detected 60 objects close to the centre of NGC 3603 that are known al- ready to be early-type emission line stars. This reduces the list to 1537 objects. How these stars are distributed in terms 40 of best-fit effective temperature (or log(Teff K) as plotted) and extinction, A0, and 2MASS K magnitude is shown in 20 Figure1. We remind that A0 represents the monochromatic extinction at a wavelength of 5495 A.˚ 0 To focus the long list down onto the likely O star con- 6 7 8 9 10 11 12 13 14 K magnitude tent of the region at a distance D . 8 kpc, and extinction A0 . 10 magnitudes, we cut both on effective temperature Figure 1. These histograms show how the MS-II objects inside 2 2 such that log(Teff K) > 4:44 and on K magnitude such that the 1.5×1.5 deg box centred on NGC 3603, satisfying χ < 25, K < 13:0. The first cut admits objects with estimated effec- are distributed in effective temperature (top panel), extinction, tive temperatures greater than 27500 K: since O stars are A0 (middle) and K magnitude (bottom). The full sample of 1537 associated with effective temperatures exceeding ∼30000 K, stars is shaded in blue. The green bars pick out the selection with this builds in some margin for fit error. The reasoning be- logTeff > 4:44 and K < 13:0 mag. These are the focus of this study. hind the second cut is that, since MK ' −3 for an O9.5 main sequence star (Martins et al. 2005), such a star at a maximal distance of 8 kpc, with A0 = 10, would suffer no more than ∼ 1 magnitude of K extinction, resulting in an apparent magnitude of K ∼ 12:5. Setting the fainter limit of K = 13:0 again makes some allowance for error. How the up at position offsets ranging from ∼0.03 to ∼0.2 arcsec reduced sample compares with the full list from MS-II is (with a mean of ∼ 0:1 arcsec). The astrometry is "good" in illustrated in Figure1. that all of them pass the mission-recommended test of as- Next, a cross-match of the reduced list of 325 stars with trometric quality: that the renormalised unit weight error, p 2 the Gaia DR2 catalogue was undertaken. We found that u=u0(G; BP − RP ) < 1:4, where u = (χ )=(N − 5) and 292 objects with good astrometry were successfully matched u0(G; BP − RP ) is the magnitude- and colour-dependent MNRAS 000, 000{000 (0000) The O star hinterland of NGC 3603 3 N E +00.00° -00.25° -00.50° Galactic Latitude -00.75° -01.00° -01.25° 292.00° 291.50° 291.00° Galactic Longitude Figure 2.
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